How many years is the sun now, how many years does the sun have to live?

Our current Sun is in the main-sequence phase and has been around for 5 billion years.

The lifetime of the sun is about 10 billion years. There are mainly protostellar --- main-sequence stars--- red giants--- white dwarfs--- black dwarfs and several stages.

The sun has 50-6 billion years to live. The Sun is a yellow dwarf star with a lifespan of about 10 billion years, and the Sun is currently about 100 million years old, about 50-6 billion years from now, the hydrogen element of the Sun.

When all depleted, the Sun's core will collapse, causing the temperature to rise, a process that will continue until the Sun is depleted of helium.

Fusion into the element carbon.

The Sun does not have enough mass to explode into a supernova.

Instead, in about 5 billion years it will enter the red giant.

, the helium core contracts in response to gravity and heats up at the same time; The hydrogen cladding immediately adjacent to the core accelerates fusion as the temperature rises, and as a result, the heat generated continues to increase, conducting it to the outer layer, causing it to expand outward.

The structure of the sun:

According to the relative intensity of solar activity, the sun can be divided into two categories: the quiet sun and the active sun. The Tranquility Sun is a theoretically assumed spherically symmetrical hot gas sphere whose properties vary only with radius and are uniform in either sphere, with the aim of studying the general structure and general properties of the Sun.

Under this assumption, the Sun is composed of the core, the radiation zone, and the troposphere, in order from the inside out.

It is composed of photosphere, chromosphere, and corona. Below the photosphere is called the interior of the Sun; Above the photosphere is called the solar atmosphere.

The life span of the sun is estimated to be billions of years, and there should be no specific time, after all, the future is unpredictable.

The lifespan of the sun is about 10 billion years, and currently, the sun is about 4.6 billion years old. The Sun has reached middle age in the evolutionary phase of its main order.

The sun has a lifespan of 5 billion years, and humans will die when the sun is destroyed.

The sun still has about 5 billion years of life.

There is no scientific basis for this claim.

The Sun is a yellow dwarf star with a lifespan of roughly 10 billion years, and the Sun is currently about 100 million years old.

After about 50 to 6 billion years, the Sun's interior will be almost completely depleted, at which point the Sun will become a red giant for a short time, then gradually cool down and eventually become a white dwarf.

Scientists now calculate that the sun has about 5 billion years left to live. So far, the Sun has passed half of its lifespan, and in about 1 billion years, the Sun may evolve into a red giant, when the Sun is too large and the Earth will lack water and there may be no life on Earth.

In order to calculate how much life the sun has left, scientists need to first estimate the total life of the sun, using physical formulas to calculate that the sun has a lifetime of about 10.4 billion years.

It is often said that the total life of the sun is 10 billion years, because the actual rate of nuclear fusion reaction of the sun is expected to be faster and faster.

The formation of the Sun can be traced back to a star-pure tremor cloud about 4.6 billion years ago. According to the now widely accepted theory, the nebula of the cave at that time was caused by the death of some huge stars that released large amounts of matter and energy in **. These matter and energy began to clump together to form a rotating cloud of gas called the primordial solar cloud.

Gradually, the material in the primordial solar cloud began to clump together, forming a huge melting sphere of very high density and temperature. Over time, the sphere experienced high-speed rotation and gravitational collapse, gradually forming a core, which we now call the sun. The temperature and pressure inside the sun's core reach a high enough level that a nuclear fusion reaction begins to take place, converting hydrogen into helium, releasing enormous amounts of energy in the process.

The formation of the sun is part of the formation of the Earth and other planets. As the material left over from the formation of the sun gradually gathers together, they form planets and other celestial bodies. According to this theory, we can assume that the Sun and other planets formed at the same time about 4.6 billion years ago.

The Sun was formed about 100 million years ago in a cloud of collapsed hydrogen molecules. The time of the formation of the Sun is measured in two ways: the current age of the Sun in the main sequence zone, which is confirmed by a computer model of the evolution of the stars and the synthesis of the primordial nucleus, which is about 100 million years.

This is very consistent with the radioactive dating of the oldest material of the sun is 100 million years old. The Sun has reached middle age in the evolutionary phase of its main sequence, in which nuclear fusion is the fusion of hydrogen into helium at the core.

Every second, more than 4 million tons of matter are converted into energy in the core of the sun, producing neutrinos and solar radiation. At this rate, so far, the sun is approximately transformed.

The sun is about 100 million years old.

The Sun is the central body of the solar system and occupies the overall mass of the solar system. The eight planets in the solar system, asteroids, meteors, comets, outer Neptune objects, and interstellar dust all revolve around the Sun, which revolves around the center of the Milky Way.

The Sun is a star located at the center of the solar system, and it is almost an ideal sphere intertwined with hot plasma and magnetic fields. The diameter of the Sun is about 1,392,000 (kilometers, equivalent to 109 times the diameter of the Earth; It is about 1.3 million times the size of the Earth; Its mass is about 2 10 kilograms (330,000 times that of the Earth).

The age of the Sun is about 4.6 billion years, and it can continue to burn for about 5 billion years The Sun is the closest star to the Earth, and it is medium in size and brightness, and it should be classified as a type G1 dwarf star in terms of radius and temperature. With a magnetic field and rotation, it is the largest celestial body and contains nearly 98% of the mass of the solar system. It would take one hundred and nine Earths to fill the cross-section of the Sun, while its interior could hold more than 1.3 million Earths.

The visible bright surface is called the photosphere, and above the photosphere is a 5,000-kilometer-thick inner atmosphere called the chromosphere, and above the chromosopher is an extremely thin hot corona that can extend to the Earth and beyond. The activity of the sun is at its core. The core temperature of the Sun is as high as 15 million degrees Celsius, and the pressure is more than 34 billion times that of the Earth.

Nuclear fusion is happening here. Fusion causes four protons or hydrogen atoms to produce an alpha particle or helium nucleus. The mass of the alpha particle is smaller than that of four protons, and the remaining mass is converted into energy and released to the surface of the sun, where it emits light and heat through the convection process.

It takes millions of years for the energy of the sun's core to reach its surface. Every second, 700 million tons of hydrogen are converted into helium. In the process, about five million tons of net energy are released, thus enabling the sun to shine.

The age of the Sun is about 4.6 billion years, and it can continue to burn for about 5 billion years. In the final stages of its existence, the helium in the Sun will be transformed into a heavy element, and the Sun's volume will begin to expand until it engulfs the Earth. After a 100 million year red giant phase, the Sun will suddenly collapse into a white dwarf - the final stage of all star existence.

After a few more trillions of years, it will finally cool down completely.

Asked some questions that no one knows

The sun will disappear in at least 6 billion years.

The sun will have an end to this day because it also has its own lifespan.

The Sun is a yellow dwarf (spectrum G2V), the lifespan of a yellow dwarf is roughly 10 billion years, and the Sun is currently about 100 million years old. In about 50 to 6 billion years, the Sun's interior will be almost completely depleted of hydrogen and the Sun's core will collapse, causing the temperature to rise, a process that will continue until the Sun begins to fuse helium into carbon. Although helium fusion produces less energy than hydrogen fusion, it is also hotter, so the outer layers of the sun will expand and release a portion of the outer atmosphere into space.

At the end of the process of turning to new elements, the mass of the Sun will decrease slightly, and the outer layers will extend to the current orbit of the Earth or Mars (at which point the two planets will be farther away from the Sun due to the decrease in the mass of the Sun).

The Sun does not have enough mass to explode into a supernova, and instead, in about 5 billion years it will enter the phase of a red giant, with the helium core contracting to resist gravity and heating at the same time; The hydrogen cladding immediately adjacent to the core accelerates fusion as the temperature rises, and as a result, the heat generated continues to increase, conducting it to the outer layer, causing it to expand outward. When the temperature of the core reaches 100 million K, helium fusion will begin and burn to produce carbon. Since the helium core at this time is already equivalent to a small "white dwarf" (electron degeneracy), thermal runaway helium fusion will cause helium flash, and the huge energy released will greatly expand the solar core, lifting the electron degeneracy, and then the remaining helium in the core will undergo stable fusion.

Externally, the Sun will suddenly brighten by 5 10 magnitudes like a nova (compared to the previous "red giant" phase), and then shrink dramatically, becoming much fainter than the original red giant (but still brighter than the current Sun) until the carbon in the core accumulates and enters the core contraction and outer expansion again. This is the asymptotic superstar branching phase.

Following the red giant phase, intense thermal pulsations will cause gas from the Sun's outer layers to escape, forming planetary nebulae. After the outer layers were stripped away, the only thing that remained was the scorching core of the star, the white dwarf, which gradually cooled and dimmed over billions of years. This is typical of low-mass vs. intermediate-mass star evolution.

You disappeared and he didn't disappear.